adsabs/AstroCLIMB huggingface dataset:
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: The apparent magnitudes reconstructed through the Gaussian process from SNe Ia data at z ≤ 2.3 (left panel), and those reconstructed from SNe Ia data at z < 1.4 (right panel). The blue curves present the reconstructed function with the 1σ uncertainty from the SNe Ia data (red dots). The apparent magnitudes of GRBs at z < 1.4 (black dots) are reconstructed from SNe Ia through the Gaussian process. The dashed line denotes z = 1.4.
Paper: One-dimensional Numerical Study on Ignition of the Helium Envelope in Dynamical Accretion during the Double-degenerate Merger
Authors: Kazuya Iwata, Keiichi Maeda
Figure caption: The left panel shows the evolution paths of the temperature/density of the envelope base for the case 11H4S (green) and 11H4L (red). The ignition condition is denoted by a star symbol. The right panel shows the temporal profiles of the base density for the two cases.
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Constraints on Ωm in the ΛCDM model at high redshift z > 1.4 only with 140 GRBs (left panel), and 98 GRBs (right panel). H 0 is set to be 70 km s−1 Mpc−1.
Paper: One-dimensional Numerical Study on Ignition of the Helium Envelope in Dynamical Accretion during the Double-degenerate Merger
Authors: Kazuya Iwata, Keiichi Maeda
Figure caption: A graphical summary of the ignition regimes illustrated in the M core–M env plane. It is shown separately for four different combinations of the composition of the primary envelope and the accretion rate. There are five ignition regimes observed: detonation (a red star), shocked subsonic flame (orange squares), isobaric ignition (black triangles), no ignition (gray bars), and the cases in which detonation occurs without the limiter, but shocked subsonic flame is obtained instead with the limiter of ΔlnT max = 0.20 (red circles).
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: GRB Hubble diagram with the A219 sample (left panel) and the A118 sample (right panel). The GRBs at z < 1.4 are obtained by a Gaussian process from SNe Ia data (purple dots), and the GRBs at z > 1.4 (blue dots) are obtained with the Amati relation calibrated with the sample at z < 1.4. The solid green curve is the CMB standard distance modulus with H 0 = 67.36 km s−1 Mpc−1, Ωm = 0.315 (Plank Collaboration et al. 2020), and the green long dotted curve is the SNIa standard distance modulus with H 0 = 74.3 km s−1 Mpc−1, Ωm = 0.298 (Scolnic et al. 2018). The black dashed line denotes z = 1.4.
Paper: Calibrating Gamma-Ray Bursts by Using a Gaussian Process with Type Ia Supernovae
Authors: Nan Liang, Zihao Li, Xiaoyao Xie, Puxun Wu
Figure caption: Calibration results (a and b) of the Amati relation at z < 1.4 and the absolute magnitude M of the Pantheon sample fitted by emcee with GRB data A220 (left panel) and A118 (right panel), respectively.
Paper: Is the Hot, Dense Sub-Neptune TOI-824 b an Exposed Neptune Mantle? Spitzer Detection of the Hot Dayside and Reanalysis of the Interior Composition
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Ian J. M. Crossfield, Laura Kreidberg, Diana Dragomir, Drake Deming, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Courtney D. Dressing, Stephen R. Kane, Farisa Y. Morales
Figure caption: Left: mass–radius measurements of small exoplanets compared to theoretical curves from interior models for different compositions. TOI-824 b is shown in yellow with 1σ error bars (Burt et al. 2020); all other confirmed exoplanets with precise mass measurements (<20%) are shown in light gray. Composition curves are shown for a range of interior compositions including 100% iron, 100% dry Earth-like interior, and 100% MgSiO3 (for T = 1000 K; Zeng et al. 2016, 2019), as well as for a 100% water composition and for a rock/iron core with icy mantle (50% Earth-like core +50% H2O mantle) (for T = 1253 K; Aguichine et al. 2021). In addition, scenarios with 1% or 2% H2/He envelopes are shown for both the dry Earth-like interior as well as for the “rocky core plus icy mantle” scenario using a temperature of 1000 K (Zeng et al. 2016, 2019). The solar system planet Neptune is added as a reference along with a hypothetical Neptune-like planet that lost its gaseous H2/He envelope (core and mantle only). TOI-824 b’s mass and radius are consistent with an exposed Neptune mantle without H2/He envelope (50% Earth-like core +50% H2O mantle) as well as with a dry Earth-like interior with 1% H2/He on the other extreme. Right: two-dimensional joint posterior density distribution for the mass fraction of water in TOI-824 b’s core and mantle (horizontal axis) and the mass fraction of a possible H2/He gaseous envelope on TOI-824 b (vertical axis). The shading represents the probability density, with the black curves indicating the 68.2%, 95.4%, and 99.7% Bayesian credible regions. The interior water mass fraction ranges from 0 (core with Earth-like composition) to 1 (pure water interior). The mass fraction of the H2/He envelope is shown on a log scale, with negligible amounts of H2/He toward the bottom of the diagram. Schematics illustrate the planet structure at the two extreme ends of the high-probability region.
Paper: Is the Hot, Dense Sub-Neptune TOI-824 b an Exposed Neptune Mantle? Spitzer Detection of the Hot Dayside and Reanalysis of the Interior Composition
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Ian J. M. Crossfield, Laura Kreidberg, Diana Dragomir, Drake Deming, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Courtney D. Dressing, Stephen R. Kane, Farisa Y. Morales
Figure caption: Left: Spitzer secondary-eclipse depth measurements (black points) compared to model secondary-eclipse spectra of TOI-824 b. Dashed lines show blackbody eclipse spectra for different dayside brightness temperatures corresponding to different combinations of low or high Bond albedos (A B = 0 and A B = 0.4) and complete or poor heat redistribution across the surface of the planet (f = 0.25 and f = 0.666). Theoretical model eclipse spectra based on self-consistent 1D atmospheres for equivalent low or high albedos and full or poor heat redistributions are shown as solid lines in matching colors (orange, red, light blue). In addition, a model including short-wavelength absorbers TiO, SiO, and VO (green) and a water-dominated case where CO and CO2 are removed (blue) are shown. The absorption features around 4.5 μm are driven by CO and CO2 opacities. Colored circles represent the models integrated over the Spitzer bandpasses. Right: joint posterior distribution of the Bond albedo (vertical axis) and heat redistribution factor (horizontal axis) for the grid of 1D self-consistent atmosphere models. The 2D posterior is shown as colored shading, with the 1σ and 2σ credible regions indicated by black lines. Colored circles in the posterior correspond to models shown in matching colors in the spectrum. The top and right panels show the marginal distributions with the 1σ and 2σ limits of the heat redistribution factor and Bond albedo, respectively. Colored dashed lines are added along the heat redistribution axis to highlight special values for the parameter (f = 0.25, 0.5, and 0.666).
Paper: Is the Hot, Dense Sub-Neptune TOI-824 b an Exposed Neptune Mantle? Spitzer Detection of the Hot Dayside and Reanalysis of the Interior Composition
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Ian J. M. Crossfield, Laura Kreidberg, Diana Dragomir, Drake Deming, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Courtney D. Dressing, Stephen R. Kane, Farisa Y. Morales
Figure caption: Top: occurrence rates of planets with orbital periods smaller than 100 days, adapted from Fulton & Petigura (2018). Bottom panels: emission spectroscopy metrics (ESMs; Kempton et al. 2018) at 3.6 and 4.5 μm computed from the equilibrium temperature for confirmed exoplanets (circles). Exoplanets with reported secondary-eclipse measurements are shown in bold (Alonso 2018). Small planets with available Spitzer 3.6 and 4.5 μm thermal emission measurements are labeled and are shown with the reported Spitzer dayside brightness temperatures (diamonds with error bars; Demory et al. 2016; Kreidberg et al. 2019; Crossfield et al. 2020; Zieba et al. 2022; Crossfield et al. 2022). For GJ 436 b and GJ 3470b at 4.5 μm, we show the brightness temperature upper bounds as triangles (Stevenson et al. 2010; Benneke et al. 2019b). The gray area in all panels highlights the radius valley. TOI-824 b has the highest ESM in the sub-Neptune range between 2 and 4 Earth radii in both bandpasses.
Paper: Is the Hot, Dense Sub-Neptune TOI-824 b an Exposed Neptune Mantle? Spitzer Detection of the Hot Dayside and Reanalysis of the Interior Composition
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Ian J. M. Crossfield, Laura Kreidberg, Diana Dragomir, Drake Deming, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Courtney D. Dressing, Stephen R. Kane, Farisa Y. Morales
Figure caption: White-light-curve fits from the joint analysis of each set of four Spitzer eclipse observations of TOI-824 b in Channel 1 (left) and Channel 2 (right). The top panels show the best-fit light curves (black curve), with the systematics-corrected observations (blue circles) and their error bars. The middle panels show the residuals from the light-curve fits shown in the top panels. The Spitzer data points are binned to 3.33 minute intervals, and the bold black points show the combination of all the data binned by groups of 100 points. In the bottom panels, the residuals divided by the photometric scatter for each eclipse are shown as histograms along with the expected Gaussian curve. The error distribution follows the expected Gaussian distribution.
Paper: Is the Hot, Dense Sub-Neptune TOI-824 b an Exposed Neptune Mantle? Spitzer Detection of the Hot Dayside and Reanalysis of the Interior Composition
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Ian J. M. Crossfield, Laura Kreidberg, Diana Dragomir, Drake Deming, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Courtney D. Dressing, Stephen R. Kane, Farisa Y. Morales
Figure caption: Spitzer secondary-eclipse depth measurements (black points) compared to model secondary-eclipse spectra of TOI-824 b from the 3D GCM. The purple line shows an atmosphere with a solar composition, while the blue line shows an atmosphere for 300× the solar composition. The colored points show the GCM models integrated over the Spitzer bandpasses. Both models were integrated over a period of 250 days, and the spectrum shows a snapshot of the last day of the simulation. The Spitzer measurements are in agreement with the metal-rich model and rule out the metal-poor model, suggesting that TOI-824 b is consistent with a metal-rich atmosphere.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: (a) Energy spectrum of the undecomposed postshock turbulent velocity (left) and Alfvén velocity (i.e., magnetic field; right) at t ≈ 0.20t shock. (b) Energy spectrum of the decomposed postshock turbulent velocity (left) and magnetic field (right) at t ≈ 0.75t shock for the cases of a shallow preshock density spectrum. (c) Same as (b), but for the case of a Kolmogorov density spectrum. Note that we consider the energy spectrum only on the k  x  = 0 plane in Fourier space. Therefore, we have the slope ≈−4 + (D − 1) and ≈−11/3 + (D − 1) for compressive and solenoidal turbulence, respectively. Here D = 2 stands for the case of a 2D spectrum. α is the slope of the preshock density distribution’s spectrum.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Left: the 2D cross sections of gas density, total velocity, magnetic field, and pressure at z = 256. The snapshot of model “Para.” at t ≈ 0.75t shock is used here. The preshock mean magnetic field is parallel to the x-axis. Short white lines indicate the magnetic field orientations. Right: averaged (over y-axis and z-axis) profiles of the gas density, total velocity, magnetic field, and pressure as functions of x using the same simulation. The physical variables are expressed in terms of numerical units.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: The anisotropy degree of velocity and magnetic field fluctuations. Here we define r  v  = 2δ v  x /(δ v  y  + δ v  z ) and r  B  = 2δ B  x /(δ B  y  + δ B  z ). The fluctuations are calculated over the postshock’s turbulent shell.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Energy spectrum of undecomposed postshock turbulent velocity and Alfvén velocity using the “Para.” model. Note that we consider the spectrum only on the k  x  = 0 plane in Fourier space. Therefore, we have the slope ≈−11/3 + (D − 1) for solenoidal turbulence. Here D = 2 stands for the case of a 2D spectrum.
Paper: Inpainting Hydrodynamical Maps with Deep Learning
Authors: Faizan G. Mohammad, Francisco Villaescusa-Navarro, Shy Genel, Daniel Anglés-Alcázar, Mark Vogelsberger
Figure caption: Ratio between the power spectra estimated using the model output and the ground truth averaged over 15,000 maps. Shaded bands show the corresponding errors on the mean. The horizontal bands delimit the 1%, 3%, and 5% intervals around the reference. Results are shown for six different auxiliary fields not used in the network training process. This result indicates that the model trained on the temperature maps fails to accurately reconstruct the masked pixels when applied to a different field. The degree at which it fails also varies from field to field.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Distribution of projected decomposed turbulent velocity. Top: the solenoidal component averaged along the z-axis. Bottom: the compressive component averaged along the z-axis. The simulation cubes “Para.” (left), “Kol.” (middle), and “Perp.” (right) at t ≈ 0.75t shock are used here. The streamlines indicate velocity directions.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Distribution of projected decomposed turbulent magnetic fields. Top: the solenoidal component averaged along the z-axis. Bottom: the compressive component averaged along the z-axis. The simulation cubes “Para.” (left), “Kol.” (middle), and “Perp.” (right) at t ≈ 0.75t shock are used here.
Paper: Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Yue Hu, Siyao Xu, James M. Stone, Alex Lazarian
Figure caption: Spectra of initial preshock density fluctuations. Blue and red lines correspond to shallow and Kolmogorov density spectra, respectively.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Measured time evolutions of normalized numbers (﹩{n}_{x}(t)/{n}_{{{\rm{\Sigma }}}_{0}}﹩) of N+, ND+, ﹩{\mathrm{ND}}_{2}^{+}﹩, ﹩{\mathrm{ND}}_{3}^{+}﹩, ﹩{\mathrm{ND}}_{4}^{+}﹩, ﹩{{\rm{D}}}_{3}^{+}﹩, and N2D+ ions in the ion trap filed with a mixture of He and D2 gas after the injection of N+ ions from the SIS. The collisional temperature is T = 209 K, the number density of deuterium gas is [g - D2] = 3.3 × 1011 cm−3, and the helium number density is [He] = 1.9 × 1013 cm−3. The fitted solution of the corresponding system of the rate equations is indicated with the solid lines. The dotted line indicates the time evolution of the normalized total number of ions in the trap, ﹩{\rm{\Sigma }}(t)={\sum }_{x}{n}_{x}(t)/{n}_{{{\rm{\Sigma }}}_{0}}﹩.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Schematic diagram of the linear 22-pole RF ion trap. See text for a detailed description and explanation of the abbreviations.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: The recovery of redshift from our fitting pipeline. The left column shows the recovery results for all the SNe Ia in our simulation, whereas the right column is restricted to only those SNe whose spectra contain no blended light from the host galaxy. The error bars have been suppressed for clarity. The top panels show the inferred redshift vs. the true redshift, and the bottom panels show the residuals defined by (z inferred − z true)/(1 + z true). The colors of the points denote the different exposure times as shown in the legend.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Efficiency of recovering redshifts as a function of SN magnitude in F106 for the entire simulated prism spectroscopic sample of 1698 SNe Ia. The left ordinate denotes what we refer to as the redshift completeness—this is the fraction of objects within a given magnitude bin that achieve a redshift accuracy of ﹩{\sigma }_{z}=\left|{\rm{\Delta }}z/(1+z)\right|\leqslant 0.01﹩. The top abscissa provides a guide to the reader as to the approximate redshift for the SN F106 magnitude; the SN redshift shown is derived under the assumption of peak phase and no intervening dust. The background histogram in gray shows the magnitude distribution of the simulated SNe Ia, with the number of objects indicated on the right-hand ordinate. The points joined by dashed lines show the measured redshift completeness from our simulation (compiled from redshifts measured for individual SNe), with colors corresponding to different exposure times as shown in the legend. The solid lines are sigmoid function fits to the measured redshift completeness points. The 50% redshift completeness magnitude for a given exposure time is denoted by m  c  in the legend.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Examples of SN Ia prism spectra that are blended with host galaxy spectra. The input high-resolution template spectra are in blue for the SN and red for the host galaxy. Extracted SN spectra are in black with gray errors. Host galaxy and SN redshifts, as well as F106 magnitudes, are shown in the legend. From top to bottom the extent of blending increases. Panel (a) shows an example of mild blending—SN Ia features are easily identifiable, and host galaxy features are largely absent in the extracted SN spectrum. Panels (b) and (c) show moderate blending—both SN Ia and host galaxy features can be identified in the SN spectrum. Panel (d) shows extreme blending between SN and host galaxy—SN Ia features are largely absent, and host galaxy features dominate in the SN spectrum. This “classification” of the extent of blending (as mild, moderate, or extreme) is qualitative—we do not attempt here to quantify the extent of the blending.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: The recovery from our fitting pipeline for phase (top row) and dust extinction (bottom row). Similar to Figure 5, the left column shows the recovery results for all the SNe Ia in our simulation, whereas the right column is restricted to only those SNe whose spectra contain no blended light from the host galaxy. The panels show the inferred value vs. the true value on the top and the difference between the inferred and true values on the bottom.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Fitted parameter residuals vs. S/N of observed spectrum for redshift (top), phase (middle), and AV (bottom). Shaded exponential curves enclose ±1σ of the residuals. For clarity, only a small subset of the SNe unaffected by blending are shown. The S/N is computed for the entire prism spectrum using the DER-SNR algorithm of Stoehr et al. (2008). The colors are the same as those used in Figure 5.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Dispersed prism image cutouts and extracted spectra for an example pair of SN and its host galaxy. The subpanels in panel (a) show a portion of the direct image (for a single detector, ≈600 × 450 pixels) and corresponding dispersed images at our three position angles. The dispersed images also highlight the regions used by pyLINEAR to extract the SN and host galaxy spectra. Panel (b) shows the extracted SN spectrum, along with the input templates for the SN and host galaxy. The exposure time for the 2D dispersed images and the 1D extracted spectra shown is 1200 s. For this particular example the pixels between the SN and host galaxy do not overlap within the segmentation map.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Estimate of the sensitivity of the Roman P127 prism, along with the HST Wide Field Camera 3 IR grisms G102 and G141, in the +1 order.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Schematic representation of the steps in our simulation pipeline. A short description of the details in each step is also given. Each box also provides, if applicable, a section/table number where it is described in detail in the text.